Signatures of stellar collapse in electron-type neutrinos

Details Signatures of stellar collapse in electron-type neutrinos Signatures of stellar collapse in electron-type neutrinos

Jan 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983natur.301..315b&link_type=abstract

Nature, vol. 301, Jan. 27, 1983, p. 315-318.

Astronomy and Astrophysics

Astronomy

28

Gravitational Collapse, Neutrinos, Neutron Stars, Stellar Evolution, Black Holes (Astronomy), Corpuscular Radiation, Electron Capture, Pulsars, Shock Wave Interaction, Stellar Mass Ejection, Stellar Radiation, Supermassive Stars, Supernovae, Thermonuclear Reactions

Scientific paper

Neutrino emissions from stellar collapse followed by a supernova or formation of a black hole are quantified in terms of the rise-time and magnitude of the leading pulse and the average energy of the neutrinos emitted. The characteristics of the pulse at the shock breakout is examined to optical depths below unity. The resulting neutrino energy is expressed in terms of the shock-strength parameter, and it is assumed that neutrinos behind the shock reach an equilibrium with the matter. Attention is given to a supernova explosion with a mass ejection, and to shock stagnation with continued accretion. In either case a continuous decrease in emission is expected down to a minimum value, due to electron capture in the newly accreted matter. All the energy of a final cold neutron star is suggested to be carried away by particle-antiparticle neutrinos, which can be detected only by their interactions with protons in water tanks. The data from the supernova or black hole formation as recorded on earth will be similar, but a secondary pulse from recollapse will arrive sooner in the stalled shock case, which would have a pulsation time of 10-20 msec.

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